DOCSLIB.ORG

Multiwavelength Star Formation Indicators: Observations1,2 H

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Multiwavelength Star Formation Indicators: Observations1,2 H The Astrophysical Journal Supplement Series, 164:52–80, 2006 May # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. MULTIWAVELENGTH STAR FORMATION INDICATORS: OBSERVATIONS1,2 H. R. Schmitt,3,4,5,6 D. Calzetti,7 L. Armus,8 M. Giavalisco,7 T. M. Heckman,7,9 R. C. Kennicutt, Jr.,10,11 C. Leitherer,7 and G. R. Meurer9 Received 2005 May 31; accepted 2005 November 13 ABSTRACT We present a compilation of multiwavelength data on different star formation indicators for a sample of nearby star forming galaxies. Here we discuss the observations, reductions and measurements of ultraviolet images obtained with STIS on board the Hubble Space Telescope (HST ), ground-based H , and VLA 8.46 GHz radio images. These observations are complemented with infrared fluxes, as well as large-aperture optical, radio, and ultraviolet data from the literature. This database will be used in a forthcoming paper to compare star formation rates at different wave bands. We also present spectral energy distributions (SEDs) for those galaxies with at least one far-infrared mea- surements from ISO, longward of 100 m. These SEDs are divided in two groups, those that are dominated by the far-infrared emission, and those for which the contribution from the far-infrared and optical emission is comparable. These SEDs are useful tools to study the properties of high-redshift galaxies. Subject headinggs: galaxies: evolution — galaxies: starburst — infrared: galaxies — radio continuum: galaxies — stars: formation — ultraviolet: galaxies 1. INTRODUCTION In recent years, all wavelength regions have been exploited to track down star formation at all redshifts and trace the star forma- The global star formation history of the universe is one of the crucial ingredients for understanding the evolution of galaxies tion history of the universe. At high redshift the Lyman-break gal- axies (Steidel et al. 1996, 1999) provide the bulk of the UV light as a whole, and for discriminating among different formation from star formation, while SCUBA has been used to detect the scenarios (Madau et al. 1998; Ortolani et al. 1995; Baugh et al. brightest FIR sources in the range 1 P z P 3 4(e.g.,Bargeretal. 1998). Star formation is traced by a number of observables, often 1999, 2000; Smail et al. 2000; Chapman et al. 2003). The Lyman- complementary to each other. The ultraviolet (UV) is where the breakgalaxiesare,byselection,activelystar-formingsystems, bulk of the energy from young, massive stars is emitted, but it resembling local starburst galaxies in many respects (Pettini et al. suffers from the effects of dust extinction. The nebular emission 1998; Meurer et al. 1997, 1999), and possibly covering a large line H is a tracer of ionizing photons, and thus of young, mas- range in metal and dust content (Pettini et al. 1999; Steidel et al. sive stars, but it is also affected by assumptions about the stellar 1999; Calzetti 1997). The SCUBA sources occupy the high end of initial mass function. The far-infrared (FIR) emission comes from the dust-processed stellar light and reliably tracks star formation in the FIR luminosity function of galaxies (Blain et al. 1999), and are dust-rich objects. The relationship between the UV-selected and moderately to very dusty galaxies, but it is not a narrowband mea- FIR-selected luminous systems is not yet clear. Whether the two surement (like the UVor H ) and needs to be measured across the typesofgalaxiesrepresenttwodistinctpopulationsorthetwo entire infrared wavelength range. Finally, the nonthermal radio ends of the same population is still subject to debate (Adelberger emission is a tracer of the supernova activity in galaxies, but suf- & Steidel 2000). The answer to this question can drastically change fers from uncertain calibration. our understanding of the evolution, star formation history, and metal/dust enrichment of galaxies. 1 Based on observations made with the NASA/ESA Hubble Space Telescope, The difficulty in relating the two types of galaxies stems from which is operated by the Association of Universities for Research in Astronomy, the paucity of simultaneous UV, H , FIR(>100 m), and radio Inc., under NASA contract NAS5-26555. 2 data for both low- and high-z galaxies. While multiwavelength Based on observations obtained with the Apache Point Observatory 3.5 m observations of high-z galaxies are hampered at present by the telescope, which is owned and operated by the Astrophysical Research Consortium. 3 Remote Sensing Division, Code 7210, Naval Research Laboratory, 4555 sensitivity and positional accuracy limitations of current instru- Overlook Avenue, Washington, DC 20375; [email protected]. mentation, multiwavelength observations of local galaxies are 4 Interferometrics, Inc., 13454 Sunrise Valley Drive, Suite 240, Herndon, VA20171. possible and are key for producing the spectral energy distribu- 5 Visiting Astronomer, Cerro Tololo Inter-American Observatory, National tions (SEDs) that can be used as templates for higher redshift Optical Astronomy Observatories, which are operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. observations. To be representative, such SEDs should cover as 6 Visiting Astronomer Kitt Peak National Observatory, National Optical As- completely as possible the parameter range of properties (metal- tronomy Observatories, which are operated by AURA, Inc., under a cooperative licity, luminosity, etc.) of galaxies. agreement with the National Science Foundation. 7 This paper presents a large, homogeneous data set of multi- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD wavelength observations of 41 local (closer than 120 Mpc) star- 21218. 8 Spitzer Science Center, California Institute of Technology, Mail Stop 220-6, forming galaxies, spanning from the UV to the radio. The UV Pasadena, CA 91125. observations are from our own HST STIS imaging centered at 9 Department of Physics and Astronomy, The Johns Hopkins University, 1600 8. The optical (H ) and radio (6 cm and 21 cm) data are Baltimore, MD 21218. from ground-based programs complementary to the HST obser- 10 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721. vations. The FIR data are from archival Infrared Astronomical 11 Institute of Astronomy, University of Cambridge, Madingley Road, Satellite (IRAS) and Infrared Space Observatory (ISO) observa- Cambridge, CB3 0HA, UK. tions spanning the wavelength range 12–200 m. 52 MULTIWAVELENGTH STAR FORMATION INDICATORS 53 TABLE 1 Sample Characteristics Velocity Distribution a ; b Name (J2000.0) (J2000.0) (km sÀ1) (Mpc) (arcmin) E(BÀV ) Morphology (1) (2) (3) (4) (5) (6) (7) (8) ESO 350-38 .................................. 0 36 52.5 À33 33 19 6132 81.8 0.5 ; 0.3 0.01 Merger NGC 232....................................... 0 42 45.8 À23 33 41 6682 89.1 1.0 ; 0.8 0.01 SB(r)a pec Mrk 555 ........................................ 0 46 05.6 À01 43 25 4156 55.4 1.4 ; 1.2 0.02 SA(rs)b pec IC 1586 ......................................... 0 47 56.1 22 22 21 5963 79.5 0.3 ; 0.3 0.02 BCG NGC 337....................................... 0 59 50.3 À07 34 44 1702 20.7 2.9 ; 1.8 0.08 SB(s)d IC 1623 ......................................... 1 07 47.2 À17 30 25 6016 80.2 0.7 ; 0.4 0.01 Merger NGC 1155..................................... 2 58 13.0 À10 21 04 4549 60.7 0.8 ; 0.7 0.04 Compact UGC 2982..................................... 4 12 22.6 05 32 51 5273 70.3 0.9 ; 0.4 0.14 Sm NGC 1569..................................... 4 30 49.3 64 50 54 40 1.6 3.6 ; 1.8 0.51 IBm NGC 1614..................................... 4 34 00.0 À08 34 45 4681 62.4 1.3 ; 1.1 0.06 SB(s)c pec NGC 1667..................................... 4 48 37.1 À06 19 13 4459 59.5 1.8 ; 1.4 0.06 SAB(r)c NGC 1672..................................... 4 45 42.1 À59 14 57 1155 14.5 6.6 ; 5.5 0.00 SB(r)bc NGC 1741..................................... 5 01 37.9 À04 15 35 3956 52.8 1.5 ; 1.0 0.06 Merger NGC 3079..................................... 10 01 57.8 55 40 49 1182 20.4 7.9 ; 1.4 0.00 SB(s)c NGC 3690..................................... 11 28 32.6 58 33 47 3121 41.6 3.0 ; 3.0 0.00 Merger NGC 4088..................................... 12 05 35.6 50 32 32 825 17.0 5.8 ; 2.2 0.00 SAB(rs)bc NGC 4100..................................... 12 06 08.7 49 34 56 1138 17.0 5.4 ; 1.8 0.01 (R’)SA(rs)bc NGC 4214..................................... 12 15 40.0 36 19 27 313 3.5 8.5 ; 6.6 0.00 IAB(s)m NGC 4861..................................... 12 59 00.3 34 50 48 880 17.8 4.0 ; 1.5 0.01 SB(s)m: NGC 5054..................................... 13 16 58.4 À16 38 03 1630 27.3 5.1 ; 3.0 0.03 SA(s)bc NGC 5161..................................... 13 29 14.4 À33 10 29 2247 33.5 5.6 ; 2.2 0.04 SA(s)c: NGC 5383..................................... 13 57 05.0 41 50 44 2333 37.8 3.2 ; 2.7 0.00 (R’)SB(rs)b:pec Mrk 799 ........................................ 14 00 45.8 59 19 44 3157 42.1 2.2 ; 1.1 0.00 SB(s)b NGC 5669..................................... 14 32 44.1 09 53 24 1387 24.9 4.0 ; 2.8 0.01 SAB(rs)cd NGC 5676..................................... 14 32 46.8 49 27 30 2237 34.5 4.0 ; 1.9 0.01 SA(rs)bc NGC 5713..................................... 14 40 11.3 À00 17 26 1872 30.4 2.8 ; 2.5 0.03 SAB(rs)bc pec NGC 5860..................................... 15 06 33.4 42 38 29 5520 73.6 1.0 ; 1.0 0.01 Peculiar NGC 6090....................................
Load more

Recommended publications
  • CO Multi-Line Imaging of Nearby Galaxies (COMING) IV. Overview Of
    Publ. Astron. Soc. Japan (2018) 00(0), 1–33 1 doi: 10.1093/pasj/xxx000 CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project Kazuo SORAI1, 2, 3, 4, 5, Nario KUNO4, 5, Kazuyuki MURAOKA6, Yusuke MIYAMOTO7, 8, Hiroyuki KANEKO7, Hiroyuki NAKANISHI9 , Naomasa NAKAI4, 5, 10, Kazuki YANAGITANI6 , Takahiro TANAKA4, Yuya SATO4, Dragan SALAK10, Michiko UMEI2 , Kana MOROKUMA-MATSUI7, 8, 11, 12, Naoko MATSUMOTO13, 14, Saeko UENO9, Hsi-An PAN15, Yuto NOMA10, Tsutomu, T. TAKEUCHI16 , Moe YODA16, Mayu KURODA6, Atsushi YASUDA4 , Yoshiyuki YAJIMA2 , Nagisa OI17, Shugo SHIBATA2, Masumichi SETA10, Yoshimasa WATANABE4, 5, 18, Shoichiro KITA4, Ryusei KOMATSUZAKI4 , Ayumi KAJIKAWA2, 3, Yu YASHIMA2, 3, Suchetha COORAY16 , Hiroyuki BAJI6 , Yoko SEGAWA2 , Takami TASHIRO2 , Miho TAKEDA6, Nozomi KISHIDA2 , Takuya HATAKEYAMA4 , Yuto TOMIYASU4 and Chey SAITA9 1Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 2Department of Cosmosciences, Graduate School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 3Department of Physics, School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 4Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 5Tomonaga Center for the History of the Universe (TCHoU), University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 6Department of Physical Science, Osaka Prefecture University, Gakuen 1-1,
    [Show full text]
  • June 2013 BRAS Newsletter
    www.brastro.org June 2013 What's in this issue: PRESIDENT'S MESSAGE .............................................................................................................................. 2 NOTES FROM THE VICE PRESIDENT ........................................................................................................... 3 MESSAGE FROM THE HRPO ...................................................................................................................... 4 OBSERVING NOTES ..................................................................................................................................... 6 MAY ASTRONOMICAL EVENTS .................................................................................................................... 9 PRESIDENT'S MESSAGE Greetings Everyone, Summer is here and with it the humidity and bugs, but I hope that won't stop you from getting out to see some of the great summer time objects in the sky. Also, Saturn is looking quite striking as the rings are now tilted at a nice angle allowing us to see the Casini Division and shadows on and from the planet. Don't miss it! I've been asked by BREC to make sure our club members are all aware of the Park Rules listed on BREC's website. Many of the rules are actually ordinances enacted by the city of Baton Rouge (e.g., No smoking permitted in public areas, No alcohol brought onto or sold on BREC property, No Gambling, No Firearms or Weapons, etc.) Please make sure you observe all of the Park Rules while at the HRPO and provide good examples for the general public. (Many of which are from outside East Baton Rouge Parish and are likely unaware of some of the policies.) For a full list of BREC's Park Rules, you may visit their Park Rules section of their website at http://brec.org/index.cfm/page/555/n/75 I'm sorry I had to miss the outing to LIGO, but it will be good to see some folks again at our meeting on Monday, June 10th.
    [Show full text]
  • Comprehensive Broadband X-Ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/Luminous Infrared Galaxies Observed with Nustar And/Or Swift/BAT
    Draft version July 26, 2021 Typeset using LATEX twocolumn style in AASTeX631 Comprehensive Broadband X-ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/luminous Infrared Galaxies Observed with NuSTAR and/or Swift/BAT Satoshi Yamada ,1 Yoshihiro Ueda ,1 Atsushi Tanimoto ,2 Masatoshi Imanishi ,3, 4 Yoshiki Toba ,1, 5 Claudio Ricci ,6, 7, 8 and George C. Privon 9 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan 2Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan 3National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan 4Department of Astronomical Science, Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan 5Research Center for Space and Cosmic Evolution, Ehime University, 2-5 Bunkyo-cho, Matsuyama, Ehime 790-8577, Japan 6N´ucleo de Astronom´ıade la Facultad de Ingenier´ıa,Universidad Diego Portales, Av. Ej´ercito Libertador 441, Santiago, Chile 7Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People's Republic of China 8George Mason University, Department of Physics & Astronomy, MS 3F3, 4400 University Drive, Fairfax, VA 22030, USA 9National Radio Astronomy Observatory, 520 Edgemont Rd, Charlottesville, VA 22903, USA (Received April 13, 2021; Revised June 11, 2021; Accepted Jul, 2021) ABSTRACT We perform a systematic X-ray spectroscopic analysis of 57 local ultra/luminous infrared galaxy systems (containing 84 individual galaxies) observed with Nuclear Spectroscopic Telescope Array and/or Swift/BAT. Combining soft X-ray data obtained with Chandra, XMM-Newton, Suzaku and/or Swift/XRT, we identify 40 hard (>10 keV) X-ray detected active galactic nuclei (AGNs) and con- strain their torus parameters with the X-ray clumpy torus model XCLUMPY (Tanimoto et al.
    [Show full text]
  • Observing Galaxies in Pegasus 01 October 2015 23:07
    Observing galaxies in Pegasus 01 October 2015 23:07 Context As you look towards Pegasus you are looking below the galactic plane under the Orion spiral arm of our galaxy. The Perseus-Pisces supercluster wall of galaxies runs through this constellation. It stretches from RA 3h +40 in Perseus to 23h +10 in Pegasus and is around 200 million light years away. It includes the Pegasus I group noted later this document. The constellation is well placed from mid summer to late autumn. Pegasus is a rich constellation for galaxy observing. I have observed 80 galaxies in this constellation. Relatively bright galaxies This section covers the galaxies that were visible with direct vision in my 16 inch or smaller scopes. This list will therefore grow over time as I have not yet viewed all the galaxies in good conditions at maximum altitude in my 16 inch scope! NGC 7331 MAG 9 This is the stand out galaxy of the constellation. It is similar to our milky way. Around it are a number of fainter NGC galaxies. I have seen the brightest one, NGC 7335 in my 10 inch scope with averted vision. I have seen NGC 7331 in my 25 x 100mm binoculars. NGC 7814 - Mag 10 ? Not on observed list ? This is a very lovely oval shaped galaxy. By constellation Page 1 NGC 7332 MAG 11 / NGC 7339 MAG 12 These galaxies are an isolated bound pair about 67 million light years away. NGC 7339 is the fainter of the two galaxies at the eyepiece. I have seen NGC 7332 in my 25 x 100mm binoculars.
    [Show full text]
  • In IAU Symp. 193, Wolf-Rayet Phenomena in Stars and Starburst
    Synthesis Models for Starburst Populations with Wolf-Rayet Stars Claus Leitherer Space Telescope Science Institute1, 3700 San Martin Drive, Baltimore, MD 21218 Abstract. The prospects of utilizing Wolf-Rayet populations in star- burst galaxies to infer the stellar content are reviewed. I discuss which Wolf-Rayet star features can be detected in an integrated stellar pop- ulation. Specific examples are given where the presence of Wolf-Rayet stars can help understand galaxy properties independent of the O-star population. I demonstrate how populations with small age spread, such as super star clusters, permit observational tests to distinguish between single-star and binary models to produce Wolf-Rayet stars. Different synthesis models for Wolf-Rayet populations are compared. Predictions for Wolf-Rayet properties vary dramatically between individual models. The current state of the models is such that a comparison with starburst populations is more useful for improving Wolf-Rayet atmosphere and evo- lution models than for deriving the star-formation history and the initial mass function. 1. Wolf-Rayet Signatures in Young Populations The central 30 Doradus region has the highest concentration of Wolf-Rayet (WR) stars in the LMC. Parker et al. (1995) classify 15 stars within 2000 (or 5 pc) of R136 as WR stars, including objects which may appear WR-like due to very dense winds (de Koter et al. 1997). This suggests that about 1 out of 10 ionizing stars around R136 is of WR type. The WR stars can be seen in an ultraviolet (UV) drift-scan spectrum of the integrated 30 Dor population obtained by Vacca et al.
    [Show full text]
  • Interacting Galaxy NGC 7714
    National Aeronautics and Space Administration Interacting Galaxy NGC 7714 Signs of a Galactic Encounter In this Hubble Space Telescope image, the tangled shape of the spiral galaxy NGC 7714 provides evidence of a dramatic encounter with another galaxy. Several features indicate a dynamic history. Perhaps most prominent is the ring-like structure that arcs around the left side of the galaxy. This golden loop, composed of older, intermediate-mass stars (like our sun) appears to extend into a faint tail stretching off to the right. The galaxy also includes two bright blue tails where vibrant star formation is occurring. One blue tail is below the galaxy’s center and leads toward the right; the other is above the center and leads off the image to the left. C Following that upper tail leads to the explanation for the distorted structures. B The tail becomes part of a bridge of material connecting to the smaller galaxy, A NGC 7715 (see inset image). By studying their shapes and star formation, astronomers have deduced that the two galaxies swung closely past each other about 100 million to 200 million years ago. Together, the odd-looking pair of galaxies is called Arp 284, after their catalog number in Halton Arp’s Atlas of Peculiar Galaxies. The universe contains many examples of galaxies that are stretched, pulled, A Tale of Two Galaxies and distorted in gravitational tug-of-wars between bypassing galaxies. Such The two galaxies that make up Arp 284 are shown in this wide view, close encounters also can compress interstellar gas clouds to spark intense star taken by a ground-based telescope.
    [Show full text]
  • ASTRONOMY and ASTROPHYSICS Young Massive Star Clusters in Nearby Spiral Galaxies? III
    Astron. Astrophys. 354, 836–846 (2000) ASTRONOMY AND ASTROPHYSICS Young massive star clusters in nearby spiral galaxies? III. Correlations between cluster populations and host galaxy properties S.S. Larsen1,2 and T. Richtler3,4 1 Copenhagen University Astronomical Observatory, Juliane Maries Vej 32, 2100 Copenhagen Ø, Denmark 2 UCO/Lick Observatory, Kerr Hall, UC Santa Cruz, CA 95064, USA ([email protected]) 3 Sternwarte der Universitat¨ Bonn, Auf dem Hugel¨ 71, 53121 Bonn, Germany 4 Grupo de Astronom´ıa, Departamento de F´ısica, Casilla 160-C, Universidad de Concepcion,´ Concepcion,´ Chile ([email protected]) Received 16 August 1999 / Accepted 22 December 1999 Abstract. We present an analysis of correlations between in- the Magellanic Clouds. It was noted early on that the Clouds, in tegrated properties of galaxies and their populations of young particular the LMC, contain a number of very massive, young massive star clusters. Data for 21 nearby galaxies presented by clusters that do not have any counterparts in our own galaxy Larsen & Richtler (1999) are used together with literature data (van den Bergh 1991; Richtler 1993). Many recent studies have for 10 additional galaxies, spanning a range in specific U-band shown the presence of such “Young Massive Clusters” (YMCs) cluster luminosity TL(U) from 0 to 15. We find that TL(U) also in a number of mergers and starburst galaxies (see e.g. list in correlates with several observable host galaxy parameters, in Harris 1999) and it is clear that the occurrence of such objects particular the ratio of Far-Infrared (FIR) to B-band flux and the is often associated with violent star formation, leading to the surface brightness.
    [Show full text]
  • The Applicability of Far-Infrared Fine-Structure Lines As Star Formation
    A&A 568, A62 (2014) Astronomy DOI: 10.1051/0004-6361/201322489 & c ESO 2014 Astrophysics The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types? Ilse De Looze1, Diane Cormier2, Vianney Lebouteiller3, Suzanne Madden3, Maarten Baes1, George J. Bendo4, Médéric Boquien5, Alessandro Boselli6, David L. Clements7, Luca Cortese8;9, Asantha Cooray10;11, Maud Galametz8, Frédéric Galliano3, Javier Graciá-Carpio12, Kate Isaak13, Oskar Ł. Karczewski14, Tara J. Parkin15, Eric W. Pellegrini16, Aurélie Rémy-Ruyer3, Luigi Spinoglio17, Matthew W. L. Smith18, and Eckhard Sturm12 1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium e-mail: [email protected] 2 Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle Str. 2, 69120 Heidelberg, Germany 3 Laboratoire AIM, CEA, Université Paris VII, IRFU/Service d0Astrophysique, Bat. 709, 91191 Gif-sur-Yvette, France 4 UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK 5 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 6 Laboratoire d0Astrophysique de Marseille − LAM, Université Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille CEDEX 13, France 7 Astrophysics Group, Imperial College, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK 8 European Southern Observatory, Karl
    [Show full text]
  • 1987Apj. . .320. .2383 the Astrophysical Journal, 320:238-257
    .2383 The Astrophysical Journal, 320:238-257,1987 September 1 © 1987. The American Astronomical Society. AU rights reserved. Printed in U.S.A. .320. 1987ApJ. THE IRÁS BRIGHT GALAXY SAMPLE. II. THE SAMPLE AND LUMINOSITY FUNCTION B. T. Soifer, 1 D. B. Sanders,1 B. F. Madore,1,2,3 G. Neugebauer,1 G. E. Danielson,4 J. H. Elias,1 Carol J. Lonsdale,5 and W. L. Rice5 Received 1986 December 1 ; accepted 1987 February 13 ABSTRACT A complete sample of 324 extragalactic objects with 60 /mi flux densities greater than 5.4 Jy has been select- ed from the IRAS catalogs. Only one of these objects can be classified morphologically as a Seyfert nucleus; the others are all galaxies. The median distance of the galaxies in the sample is ~ 30 Mpc, and the median 10 luminosity vLv(60 /mi) is ~2 x 10 L0. This infrared selected sample is much more “infrared active” than optically selected galaxy samples. 8 12 The range in far-infrared luminosities of the galaxies in the sample is 10 LQ-2 x 10 L©. The far-infrared luminosities of the sample galaxies appear to be independent of the optical luminosities, suggesting a separate luminosity component. As previously found, a correlation exists between 60 /¿m/100 /¿m flux density ratio and far-infrared luminosity. The mass of interstellar dust required to produce the far-infrared radiation corre- 8 10 sponds to a mass of gas of 10 -10 M0 for normal gas to dust ratios. This is comparable to the mass of the interstellar medium in most galaxies.
    [Show full text]
  • Modelling Ionised and Photodissociated Regions
    Modelling ionised and photodissociated regions Magda Vasta Thesis submitted for the Degree of Doctor of Philosophy of University College London Department of Physics & Astronomy UNIVERSITY COLLEGE LONDON March 2010 I, Magda Vasta, confirm that the work presented in this thesis is my own. Where information has been derived from other sources, I confirm that this has been indicated in the thesis. To my parents, my brother and my husband, who always supported and encouraged me no matter what. I tell people I am too stupid to know what is impossible. I have ridiculously large dreams, and half the time they come true. — Thomas D. ACKNOWLEDGEMENTS Some people come into our lives and quickly go. Some stay for a while and leave footprints on our hearts. And we are never, ever the same. I made it, I still cannot believe it, but I finally made it. However, it would have been almost impossible to reach this target without the constant scientific support from some people. My first big THANKS go to my supervisor Serena Viti. Thanks for being the supportive person you are, for giving me the possibility to be independent in my research, but being always present when I needed you. Thanks for all the times that you did not talk to me in Italian, for encouraging me to not give up and for being the lovely person you are. Thanks to Mike Barlow for the amazing scientific suggestions and for tolerating ALL my silly questions (most of them grammatically incorrect!). Thanks to Barbara Ercolano for her patience when answering my emails “HELP, PLEASE!!” about MOCASSIN.
    [Show full text]
  • Lopsided Spiral Galaxies: Evidence for Gas Accretion
    A&A 438, 507–520 (2005) Astronomy DOI: 10.1051/0004-6361:20052631 & c ESO 2005 Astrophysics Lopsided spiral galaxies: evidence for gas accretion F. Bournaud1, F. Combes1,C.J.Jog2, and I. Puerari3 1 Observatoire de Paris, LERMA, 61 Av. de l’Observatoire, 75014 Paris, France e-mail: [email protected] 2 Department of Physics, Indian Institute of Science, Bangalore 560012, India 3 Instituto Nacional de Astrofísica, Optica y Electrónica, Calle Luis Enrique Erro 1, 72840 Tonantzintla, Puebla, Mexico Received 3 January 2005 / Accepted 15 March 2005 Abstract. We quantify the degree of lopsidedness for a sample of 149 galaxies observed in the near-infrared from the OSUBGS sample, and try to explain the physical origin of the observed disk lopsidedness. We confirm previous studies, but for a larger sample, that a large fraction of galaxies have significant lopsidedness in their stellar disks, measured as the Fourier amplitude of the m = 1 component normalised to the average or m = 0 component in the surface density. Late-type galaxies are found to be more lopsided, while the presence of m = 2 spiral arms and bars is correlated with disk lopsidedness. We also show that the m = 1 amplitude is uncorrelated with the presence of companions. Numerical simulations were carried out to study the generation of m = 1viadifferent processes: galaxy tidal encounters, galaxy mergers, and external gas accretion with subsequent star formation. These simulations show that galaxy interactions and mergers can trigger strong lopsidedness, but do not explain several independent statistical properties of observed galaxies. To explain all the observational results, it is required that a large fraction of lopsidedness results from cosmological accretion of gas on galactic disks, which can create strongly lopsided disks when this accretion is asymmetrical enough.
    [Show full text]
  • 00E the Construction of the Universe Symphony
    The basic construction of the Universe Symphony. There are 30 asterisms (Suites) in the Universe Symphony. I divided the asterisms into 15 groups. The asterisms in the same group, lay close to each other. Asterisms!! in Constellation!Stars!Objects nearby 01 The W!!!Cassiopeia!!Segin !!!!!!!Ruchbah !!!!!!!Marj !!!!!!!Schedar !!!!!!!Caph !!!!!!!!!Sailboat Cluster !!!!!!!!!Gamma Cassiopeia Nebula !!!!!!!!!NGC 129 !!!!!!!!!M 103 !!!!!!!!!NGC 637 !!!!!!!!!NGC 654 !!!!!!!!!NGC 659 !!!!!!!!!PacMan Nebula !!!!!!!!!Owl Cluster !!!!!!!!!NGC 663 Asterisms!! in Constellation!Stars!!Objects nearby 02 Northern Fly!!Aries!!!41 Arietis !!!!!!!39 Arietis!!! !!!!!!!35 Arietis !!!!!!!!!!NGC 1056 02 Whale’s Head!!Cetus!! ! Menkar !!!!!!!Lambda Ceti! !!!!!!!Mu Ceti !!!!!!!Xi2 Ceti !!!!!!!Kaffalijidhma !!!!!!!!!!IC 302 !!!!!!!!!!NGC 990 !!!!!!!!!!NGC 1024 !!!!!!!!!!NGC 1026 !!!!!!!!!!NGC 1070 !!!!!!!!!!NGC 1085 !!!!!!!!!!NGC 1107 !!!!!!!!!!NGC 1137 !!!!!!!!!!NGC 1143 !!!!!!!!!!NGC 1144 !!!!!!!!!!NGC 1153 Asterisms!! in Constellation Stars!!Objects nearby 03 Hyades!!!Taurus! Aldebaran !!!!!! Theta 2 Tauri !!!!!! Gamma Tauri !!!!!! Delta 1 Tauri !!!!!! Epsilon Tauri !!!!!!!!!Struve’s Lost Nebula !!!!!!!!!Hind’s Variable Nebula !!!!!!!!!IC 374 03 Kids!!!Auriga! Almaaz !!!!!! Hoedus II !!!!!! Hoedus I !!!!!!!!!The Kite Cluster !!!!!!!!!IC 397 03 Pleiades!! ! Taurus! Pleione (Seven Sisters)!! ! ! Atlas !!!!!! Alcyone !!!!!! Merope !!!!!! Electra !!!!!! Celaeno !!!!!! Taygeta !!!!!! Asterope !!!!!! Maia !!!!!!!!!Maia Nebula !!!!!!!!!Merope Nebula !!!!!!!!!Merope
    [Show full text]